Explaining temporal variations in the jet PA of the blazar OJ 287 using its BBH central engine model. Issue 3 (13th March 2021)

• Record Type: Journal Article
• Authors: Dey, Lankeswar; Valtonen, Mauri J; Gopakumar, A; Lico, Rocco; Gómez, José L; Susobhanan, Abhimanyu; Komossa, S; Pihajoki, Pauli
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 503:Issue 3(2021)
• Page Start: 4400
• Page End: 4412
• Publication Date: 2021-03-13
• Subjects: accretion, accretion discs -- BL Lacertae objects: individual: OJ 287 -- galaxies: jets -- black hole physics; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab730
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The bright blazar OJ 287 is the best-known candidate for hosting a supermassive black hole binary system. It inspirals due to the emission of nanohertz gravitational waves (GWs). Observations of historical and predicted quasi-periodic high-brightness flares in its century-long optical lightcurve, allow us to determine the orbital parameters associated with the binary black hole (BBH) central engine. In contrast, the radio jet of OJ 287 has been covered with Very Long Baseline Interferometry (VLBI) observations for only about 30 yr and these observations reveal that the position angle (PA) of the jet exhibits temporal variations at both millimetre and centimetre wavelengths. Here, we associate the observed PA variations in OJ 287 with the precession of its radio jet. In our model, the evolution of the jet direction can be associated either with the primary black hole (BH) spin evolution or with the precession of the angular momentum direction of the inner region of the accretion disc. Our Bayesian analysis shows that the BBH central engine model, primarily developed from optical observations, can also broadly explain the observed temporal variations in the radio jet of OJ 287 at frequencies of 86, 43, and 15 GHz. Ongoing Global mm-VLBI Array (GMVA) observations of OJ 287 have the potential to verify our predictions for the evolution of its 86-GHz PA values. Additionally, thanks to the extremely high angular resolution that the Event Horizon Telescope (EHT) can provide, we explore the possibility to test our BBH model through the detection of the jet in the secondary BH.